Measurement of the Crab nebula polarization at 90 GHz as a calibrator for CMB experiments

被引：66

作者：

Aumont, J. ^{[1
]}

Conversi, L. ^{[2
]}

Thum, C. ^{[3
]}

Wiesemeyer, H. ^{[4
]}

Falgarone, E. ^{[5
,6
]}

Macias-Perez, J. F. ^{[7
]}

Piacentini, F. ^{[8
]}

Pointecouteau, E. ^{[9
]}

Ponthieu, N. ^{[1
]}

Puget, J. L. ^{[1
]}

Rosset, C. ^{[10
]}

Tauber, J. A. ^{[11
]}

Tristram, M. ^{[12
]}

机构：

[1] Ctr Univ Orsay, Inst Astrophys Spatiale, F-91405 Orsay, France

[2] European Space Astron Ctr, Madrid 28691, Spain

[3] Inst Radio Astron Millimetr, F-38406 St Martin Dheres, France

[4] Inst Radio Astron Millimetr, Granada 18012, Spain

[5] Ecole Normale Super, LERMA LRA, CNRS, UMR 8112, F-75231 Paris 05, France

[6] Observ Paris, F-75231 Paris 05, France

[7] Univ Grenoble 1, CNRS IN2P3, Inst Natl Polytech Grenoble, Lab Phys Subatom & Cosmol, F-38026 Grenoble, France

[8] Univ Roma La Sapienza, Dipartimento Fis, I-00185 Rome, Italy

[9] Univ Toulouse, CNRS, Ctr Etud Spatiale Rayonnements, F-31028 Toulouse 4, France

[10] Univ Paris 07, CNRS, IN2P3, CEA,Observ Paris,APC, Paris, France

[11] European Space Agcy, Div Astrophys, NL-2201 AZ Noordwijk, Netherlands

[12] Univ Paris 11, CNRS, IN2P3, LAL, F-91898 Orsay, France

来源：

ASTRONOMY & ASTROPHYSICS | 2010年 / 514卷

关键词：

ISM: supernova remnants; polarization; cosmology: cosmic background radiation; VARIABLE RADIO-SOURCES; POWER SPECTRA; FLUX-DENSITY; CAS-A; MICROWAVE; TELESCOPE; SCALE; POLARIMETER; XPOL;

D O I：

10.1051/0004-6361/200913834

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Context. CMB experiments aiming at a precise measurement of the CMB polarization, such as the Planck satellite, need a strong polarized absolute calibrator on the sky to accurately set the detectors polarization angle and the cross-polarization leakage. As the most intense polarized source in the microwave sky at angular scales of few arcminutes, the Crab nebula will be used for this purpose. Aims. Our goal was to measure the Crab nebula polarization characteristics at 90 GHz with unprecedented precision. Methods. The observations were carried out with the IRAM 30 m telescope employing the correlation polarimeter XPOL and using two orthogonally polarized receivers. Results. We processed the Stokes I, Q, and U maps from our observations in order to compute the polarization angle and linear polarization fraction. The first is almost constant in the region of maximum emission in polarization with a mean value of alpha(Sky) = 152.1 +/- 0.3 degrees in equatorial coordinates, and the second is found to reach a maximum of Pi = 30% for the most polarized pixels. We find that a CMB experiment having a 5 arcmin circular beam will see a mean polarization angle of alpha(Sky) = 149.9 +/- 0.2 degrees and a mean polarization fraction of Pi = 8.8 +/- 0.2%.

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